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  • 1
    Electronic Resource
    Electronic Resource
    A Direct Image of the Inner Torus of NGC 1068 (1997)
    Springer
    Astrophysics and space science 248 (1997), S. 253-260 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present the first VLBI observations of the compact source S1 in the radio jet of NGC 1068. Roughly 1 pc in length and 0.2 pc wide, S1 resolves into clumps aligned perpendicular to the local radio jet axis. The radio continuum emission arises from a hot (Te ~ 106 K), dense (ne ~ 106 cm-3) plasma, and the source of the radio emission is either thermal free-free emission or Thomson-reflected synchrotron emission. The clouds comprising S1 are opaque to soft X-radiation, and we therefore propose that S1 is the inner, ionized region, or ‘hot zone,’ of the obscuring medium surrounding the active nucleus. The covering fraction of the hot zone is small, Cf ⋦ 10%. Since the covering fraction of the dusty, obscuring medium is probably much larger, the obscuring disk must either flare or warp outside of the hot zone. That the radio jet and hot zone axes are perpendicular also suggests that the hot zone may be considered to trace the outermost extent of the accretion disk.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1000502300844
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  • 2
    Electronic Resource
    Electronic Resource
    The Ringberg Standards for NGC 1068 (1997)
    Springer
    Astrophysics and space science 248 (1997), S. 9-19 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract At the end of three days' spirited discussion of the type 2 Seyfert galaxy NGC 1068, what do we think we understand about this object? New observations -- particularly in the infrared and radio -- are helping to resolve old problems, while drawing attention to new ones. It appears that NGC 1068 is a relatively normal spiral galaxy in which large-scale gravitational disturbances are funneling matter into the nucleus. A collimated outflow disturbs the interstellar medium out to kiloparsec scales, but the nucleus itself is hidden behind an opaque screen. Radio observations have now pierced the screen, and suggest that at the center of it all, a 10-20 million solar mass black hole is accreting at close to its Eddington limit.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1000567831370
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  • 3
    Electronic Resource
    Electronic Resource
    Molecular gas distribution and dynamics in the luminous merger NGC 6240 (1999)
    Springer
    Astrophysics and space science 266 (1999), S. 157-162 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present the results of our subarcsecond resolution interferometricobservations of the 1.3 mm CO J = 2→1 line in the luminous merger NGC6240. Roughly half of the CO flux is contained in a rotating and highlyturbulent thick disk centered between the two radio and near-infrarednuclei. In this disk the molecular gas has velocity widths which reachFWZP line widths of up to 1000 km s-1. The mass of this gasconcentration makes up between 30%–70% of the dynamical mass in thisregion. NGC 6240 may be in an earlier merging stage than typical ULIRGssuch as Arp 220. We compare these results from NGC 6240 with thoseof other luminous, gas-rich interacting galaxies and mergers.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1002614118115
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  • 4
    Electronic Resource
    Electronic Resource
    A High Spatial Resolution Study of the Molecular Gas in NGC 1068 (1997)
    Springer
    Astrophysics and space science 248 (1997), S. 59-66 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present preliminary results from 1.5″ resolution IRAM interferometer maps of CO 2↛1 emission in the central few arcseconds of NGC 1068. This study is unlike other studies of the CO content of this galaxy since it resolves for the first time the central dense gas concentration seen previously in HCN observations. The HCN ‘disk’ is resolved into two prominent peaks symmetrically located ~1″ from the S1 radio peak. These peaks are likely tracing gas located on x2 orbits at the Inner Lindblad Resonance (ILR). The kinematic structure is also very complex with three distinct velocity components visible in the central ~2″.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1000532218166
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